0Assigned ID: 309
----- Attempting Submission 1 (Fri Aug 17 17:03:33 GMT 2018) -----
HST Phase I Proposal 309 (proxima.apt) successfully submitted.
Receipt: # 309-1
----- Attempting Submission 2 (Fri Aug 17 22:11:07 GMT 2018) -----We would like to get a head start on assessing whether this program is schedulable as planned. We need to give information to ALMA about how to update the scheduling there and reserve the appropriate nights at Las Campanas Observatory.
The object is not bright for STIS Far-UV except when it flares. Previous observations with the same setup have not been problematic.
Resubmission on Dec 6 with the new APT 26.2.2 to fix the exposure times to fit with the new longer GS ACQs.
Visit 7 failed on a guide star acquisision and HOPR 91535 was approved to for a four orbit repeat. Resubmission on May 3 to attempt to schedule this repeat visit as Visit 12.
Visit 8 failed on a guide star acquisision and HOPR 91536 was approved to for a four orbit repeat. Resubmission on May 6 to attempt to schedule this repeat visit as Visit 13.
Visit 10 failed on a guide star acquisision and HOPR 91539 was approved to for a four orbit repeat. Resubmission on May 9 to attempt to schedule this repeat visit as Visit 60 (replacing Visit 14 from the previous submission). Visit 60 allows shorter exposure times for increased target visibility, so the target visibility window now opens May 29.
Visit 09 failed on a guide star re-acquisition on 2nd orbit. a HOPR has been submitted.
Visits 59 and 60 need to be scheduled to start at ~23:00 UT.622850004----- Attempting Submission 1 (Mon Nov 19 19:26:34 GMT 2018) -----
HST Phase II Proposal 15651 (15651_phase2.apt) successfully submitted.
Receipt: # 15651-1
----- Attempting Submission 2 (Wed Dec 05 22:51:21 GMT 2018) -----
----- Attempting Submission 3 (Thu Dec 06 17:29:52 GMT 2018) -----
----- Attempting Submission 4 (Fri May 03 19:51:38 GMT 2019) -----
----- Attempting Submission 5 (Mon May 06 19:33:44 GMT 2019) -----
HST Phase II Proposal 15651 (15651_phase2_6may19.apt) successfully submitted.
Receipt: # 15651-5
----- Attempting Submission 7 (Thu May 09 18:43:58 GMT 2019) -----
----- Attempting Submission 8 (Mon May 13 19:15:47 GMT 2019) -----
HST Phase II Proposal 15651 (Untitled.apt) successfully submitted.
Receipt: # 15651-8
----- Attempting Submission 9 (Thu May 16 20:49:10 GMT 2019) -----The Origin and Impact of Flares in the Closest Planetary System- Proxima CentauriAt a distance of only 1.3 pc, Proxima Cen is the closest extrasolar planetary system, and has long been known as a flare star, making it a benchmark case for exploring the potential effects of variability on the planet's properties. After the detection of a large millimeter flare was reported by MacGregor et al. (2018), the team was awarded 36 more hours of observations (project 2018.1.00470.S) to monitor the Proxima Cen system in 2019 with ALMA. In order to determine how stellar flaring emission correlates across the electromagnetic spectrum, simultaneous observations with other facilities across a broad range of wavelengths should be obtained along with the ALMA project. With the UV being the most critical wavelength to understand planet photochemistry and habitability, we propose to obtain simultaneous UV spectroscopy with HST in order to better constrain the properties of detected flares and their potential impact on planetary habitability. By undertaking this comprehensive, multi-wavelength monitoring campaign of Proxima Cen, we will execute the first truly panchromatic analysis of M dwarf flaring activity.At a distance of only 1.3 pc, Proxima Cen is the closest extrasolar planetary system, and has long been known as a flare star, making it a benchmark case for exploring the potential effects of variability on the planet's properties. In order to determine how stellar flaring emission correlates across the electromagnetic spectrum, we require simultaneous observations with HST and other facilities across a broad range of wavelengths. To monitor the star in the sub-mm, 41 hours of ACA/ALMA time was allocated in Cycle 6 under proposal 2018.1.00470.S to be executed in spring 2019. TESS will observe Proxima Cen in its Sector 11 between 2019 April 22 and May 21. We require simultaneous HST observations to measure far-UV flare properties. By undertaking this comprehensive, multi-wavelength monitoring campaign of Proxima Cen, we will execute the first truly panchromatic analysis of M dwarf flaring activity.
The UV observations from HST/STIS will provide the most important wavelength for understanding planet photochemistry and habitability. We will also use the UV data to measure the flare frequency distribution for Proxima to assess whether the frequent but low-energy flares or the infrequent large flares are most important to the total far-UV emission.
We will observe Proxima Cen for 11 visits of 4 orbits each with the STIS E140M grating in the 0.2 x 0.2 arcsec slit, covering 1150 - 1700 Ang. The observations are time critical to ensure simultaneity between ALMA/ACA, TESS, and HST. We therefore constrain the timing of these STIS observations first, to the TESS observations, which are inflexible, and will take place from 2019 April 22 - May 21. Second, we constrain the HST visits to take place at night in Chile so that ALMA can obtain simultaneous data. Other ground-based optical observations in Chile can then take place including white-light photometry from Evryscope and H-alpha spectroscopic monitoring at Las Campanas Observatory.
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